PSR J1833-1034 and its associated Pulsar Wind Nebula ( PWN ) has been investigated in depth through X-ray observations ranging from 0.1 to 200 keV .
The low energy X-ray data from Chandra reveal a complex morphology that is characterised by a bright central plerion , no thermal shell and an extended diffuse halo .
The spectral emission from the central plerion softens with radial distance from the pulsar , with the spectral index ranging from \Gamma = 1.61 in the central region to \Gamma =2.36 at the edge of the PWN .
At higher energy INTEGRAL detected the source in the 17–200 keV range .
The data analysis clearly shows that the main contribution to the spectral emission in the hard X-ray energy range is originated from the PWN , while the pulsar is dominant above 200 keV .
Recent HESS observations in the high energy gamma-ray domain show that PSR J1833-1034 is a bright TeV emitter , with a flux corresponding to \sim 2 per cent of the Crab in 1–10 TeV range .
In addition the spectral shape in the TeV energy region matches well with that in the hard X-rays observed by INTEGRAL .
Based on these findings , we conclude that the emission from the pulsar and its associated PWN can be described in a scenario where hard X-rays are produced through synchrotron light of electrons with Lorentz factor \gamma \sim 10 ^ { 9 } in a magnetic field of \sim 10 micro Gauss .
In this hypothesis the TeV emission is due to Inverse Compton interaction of the cooled electrons off the Cosmic Microwave Background photons .
Search for PSR J1833-1034 X-ray pulsed emission , via RXTE and Swift X-ray observations , resulted in an upper limit that is about 50 per cent .